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Surface brightness profiles for 23 M31 star clusters were measured usingimages from the Wide Field Planetary Camera 2 on the Hubble Space Telescope,and fit to two types of models to determine the clusters' structuralproperties. The clusters are primarily young (~10^8 yr) and massive (~10^4.5solar masses), with median half-light radius 7 pc and dissolution times of afew Gyr. The properties of the M31 clusters are comparable to those of clustersof similar age in the Magellanic Clouds. Simulated star clusters are used toderive a conversion from statistical measures of cluster size to half-lightradius so that the extragalactic clusters can be compared to young massiveclusters in the Milky Way. All three sets of star clusters fall approximatelyon the same age-size relation. The young M31 clusters are expected to dissolvewithin a few Gyr and will not survive to become old, globular clusters.However, they do appear to follow the same fundamental plane relations as oldclusters; if confirmed with velocity dispersion measurements, this would be astrong indication that the star cluster fundamental plane reflects universalcluster formation conditions.

An HST/WFPC2 Survey of Bright Young Clusters in M31 III. Structural Parameters